Examining the Coronal Source and Inner Heliospheric Evolution of a Stream Sampled by Parker Solar Probe and Solar Orbiter

With the growing number of solar probes across the inner heliosphere, our community, now more than ever, is well placed to continuously track the formation and supersonic expansion of the solar wind from the Sun. To capture the conditions of solar wind release connected to heliospheric structures, it is fundamental to link near-synchronous measurements of its state in the corona to the associated stream’s interplanetary propagation. This goal can be achieved through well-aligned spacecraft conjunctions, measuring local plasma conditions, with integrated remote sensing observations of the stream’s coronal birthplace. As such, this work traces a solar wind stream from its source to interplanetary space through combined remote (Solar Orbiter/FSI and SPICE, SDO/AIA, Hinode/EIS) and in situ (Parker Solar Probe, Solar Orbiter) observations of the same solar wind stream at two heliospheric distances. Using remote coverage of the source region’s thermal and elemental composition properties, the solar wind is connected throughout the heliosphere by its heavy ion composition to relate energetics of the wind at different stages of its heliospheric evolution to its source region conditions.